论文标题
h $ _2 $ o和ch $ _3 $ oh oh masers in C型冲击波的碰撞抽气
Collisional Pumping of H$_2$O and CH$_3$OH Masers in C-Type Shock Waves
论文作者
论文摘要
H $ _2 $ o和ch $ _3 $ oh oh oh oh oh masers的碰撞抽水被考虑在内。 C-Type冲击模型的网格，其速度在范围内$ 5-70 $ km s $^{ - 1} $和Preshock Gas Gusenities $ n _ {\ rm H_2,0} = 10^4-10^7 $ cm $^{ - 3} $。较大的速度梯度近似用于求解分子线中的辐射转移方程。 para-h $ _2 $ o 183.3 GHz和Ortho-h $ _2 $ o 380.1和448.0 GHz过渡已被证明是倒置的，并且在相对低的汽油密度范围内的$ N ___________2的气体密度\ sim 1 $沿冲击速度$ \ vert $ \ vert f \ vert th fert $ \ vert f \ vert \ sim。 10^5-10^6 $ cm $^{ - 3} $。较高的气体密度，$ n _ {\ rm h_2} \ gtrsim 10^7 $ cm $^{ - 3} $是有效泵送其余的H $ _2 $ o masers所需的。 Simultaneous generation of H$_2$O and class I CH$_3$OH maser emission in a shock is possible at preshock gas densities $n_{\rm H_2,0} \approx 10^5$ cm$^{-3}$ and shock speeds in the range $u_{\rm s} \approx 17.5-22.5$ km s$^{-1}$.研究了在星形区域和Supernova残留物附近检测I级$ _3 $ oh $ _3 $ oh $ _3 $ _2 $ o _2 $ _2 $ _2 $ _2 $ _3 $ _3 $ _3 $ _3 $ _3 $ _3 $ _3 $ _3的可能性。
The collisional pumping of H$_2$O and CH$_3$OH masers in magnetohydrodynamic nondissociative C-type shocks is considered. A grid of C-type shock models with speeds in the range $5-70$ km s$^{-1}$ and preshock gas densities $n_{\rm H_2,0} = 10^4-10^7$ cm$^{-3}$ is constructed. The large velocity gradient approximation is used to solve the radiative transfer equation in molecular lines. The para-H$_2$O 183.3 GHz and ortho-H$_2$O 380.1 and 448.0 GHz transitions are shown to be inverted and to have an optical depth along the shock velocity $\vert τ\vert \sim 1$ at relatively low gas densities in the maser zone, $n_{\rm H_2} \gtrsim 10^5-10^6$ cm$^{-3}$. Higher gas densities, $n_{\rm H_2} \gtrsim 10^7$ cm$^{-3}$, are needed for efficient pumping of the remaining H$_2$O masers. Simultaneous generation of H$_2$O and class I CH$_3$OH maser emission in a shock is possible at preshock gas densities $n_{\rm H_2,0} \approx 10^5$ cm$^{-3}$ and shock speeds in the range $u_{\rm s} \approx 17.5-22.5$ km s$^{-1}$. The possibility of detecting class I CH$_3$OH and para-H$_2$O 183.3 GHz masers in star-forming regions and near supernova remnants is investigated.
